Properties of the Hermean regolith: I. Global regolith albedo variation at 200 scale from multicolor CCD imaging

Warell, J.; Limaye, S. S.

doi:10.1016/s0032-0633(01)00091-5

Cited by 45 publications

(35 citation statements)

References 41 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…The true nature of the feature described as a possible volcano [Harmon, 1997] will be known once the hemisphere unimaged by Mariner 10 is finally analyzed. A preliminary map of this hemisphere is available [Warell et al, 1998]. …”

Section: Dynamicsmentioning

confidence: 99%

The surface‐bounded atmospheres of Mercury and the Moon

Killen¹,

Ip²

1999

Reviews of Geophysics

171

123

View full text Add to dashboard Cite

Abstract. Surface-bounded exospheres have been detected at the Moon, Mercury, and Europa and almost certainly exist about other objects. Historically, the first of these systems to be observed was the lunar exosphere, where He and Ar were detected by the Apollo spacecraft. The Hermean exosphere is archetypical of these systems in that it is part of a coupled system including the surface and magnetosphere interacting dynamically with the solar wind and fields. Studies of the Hermean exosphere heretofore have neglected or only superficially considered these interactions. We will review the current state of knowledge of the exospheres of Mercury and the Moon and discuss areas in which our knowledge is most incomplete. We will focus on the exosphere as part of a coupled system including the surface at its base and the particle, field, and interplanetary environment as both a source and sink for neutrals. Apollo era instruments made unambiguous detections of 36mr, 4ømr, Early Work and OverviewIn a review prior to the Mariner 10 encounter, Banks et al. [1970] reported no observational evidence for the presence of an atmosphere about Mercury. They predicted an exosphere (N < 2 x 10 TM cm -2) or thin atmosphere resulting from diffusion or effusion from the interior, solar wind implantation with subsequent thermal evaporation, or sputtering. By scaling terrestrial noble gas production and diffusion rates and assuming a lunar-like solar wind interaction, they suggested that the most abundant constituents should be the noble gases derived from the solar wind and radiogenic sources, the most abundant being 4He, followed by 4øAr and 2øNe.

show abstract

Section: Dynamicsmentioning

confidence: 99%

The surface‐bounded atmospheres of Mercury and the Moon

Killen¹,

Ip²

1999

Reviews of Geophysics

171

123

View full text Add to dashboard Cite

show abstract

“…The disk-integrated observations of Mallama et al (2002) and the diskresolved observations of Warell and Limaye (2001) support a smoother surface on Mercury. However, the Mariner 10 disk-resolved data better match a surface with the higher, lunar-like roughness values.…”

Section: Physical Properties: Photometrymentioning

confidence: 59%

“…To date these photometrically derived properties for Mercury have been studied through the analysis of both telescopic observations (Danjon 1949;de Vaucouleurs 1964;Dollfus and Auriere 1974;Mallama et al 2002;Warell and Limaye 2001) and Mariner 10 spacecraft measurements (Hapke 1984;Bowell et al 1989;. There have been several studies of Mercury's photometric properties using Hapke's (1993) model (Veverka et al 1988;Domingue et al 1997;Mallama et al 2002;Warell 2004), especially in comparison to similar studies of the Moon (Veverka et al 1988;Mallama et al 2002;Warell 2004).…”

Section: Physical Properties: Photometrymentioning

confidence: 99%

“…In addition, disk-resolved photometric measurements are now available from high-resolution CCD images obtained with the Swedish Vacuum Solar Telescope (SVST; Warell and Limaye 2001). Warell (2004) improved previous modeling efforts by simultaneously fitting both disk-integrated (Mallama et al 2002) and disk-resolved observations, using a more comprehensive Hapke model (Hapke 1981(Hapke , 1984(Hapke , 1986(Hapke , 1993(Hapke , 2002) and a Henyey-Greenstein single particle scattering function (which can be compared with the laboratory studies of particle scattering behavior versus particle structure by McGuire and Hapke 1995).…”

Section: Physical Properties: Photometrymentioning

confidence: 99%

See 1 more Smart Citation

The Geology of Mercury: The View Prior to the MESSENGER Mission

Head¹,

Chapman²,

Domingue³

et al. 2007

The Messenger Mission to Mercury

View full text Add to dashboard Cite

Mariner 10 and Earth-based observations have revealed Mercury, the innermost of the terrestrial planetary bodies, to be an exciting laboratory for the study of Solar System geological processes. Mercury is characterized by a lunar-like surface, a global magnetic field, and an interior dominated by an iron core having a radius at least three-quarters of the radius of the planet. The 45% of the surface imaged by Mariner 10 reveals some distinctive differences from the Moon, however, with major contractional fault scarps and huge expanses of moderate-albedo Cayley-like smooth plains of uncertain origin. Our current image coverage of Mercury is comparable to that of telescopic photographs of the Earth's Moon prior to the launch of Sputnik in 1957. We have no photographic images of one-half of the surface, the resolution of the images we do have is generally poor (∼1 km), and as with many lunar telescopic photographs, much of the available surface of Mercury is distorted by foreshortening due to viewing geometry, or poorly suited for geological analysis and impact-crater counting for age determinations because of high-Sun illumination conditions. Currently available topographic information is also very limited. Nonetheless, Mercury is a geological laboratory that represents (1) a planet where the presence of a huge iron core may be due to impact stripping of the crust and upper mantle, or alternatively, where formation of a huge core may have resulted in a residual mantle and crust of potentially unusual composition and structure; (2) a planet with an internal chemical and mechanical structure that provides new insights into planetary thermal history and the relative roles of conduction and convection in planetary heat loss; (3) a one-tectonic-plate planet where constraints on major interior processes can be deduced from the geology of the global tectonic system; (4) a planet where volcanic resurfacing may not have played a significant role in planetary history and internally generated volcanic resurfacing may have ceased at ∼3.8 Ga; (5) a planet where impact craters can be used to disentangle the fundamental roles of gravity and mean impactor velocity in determining impact crater morphology and morphometry; (6) an environment where global impact crater counts can test fundamental concepts of the distribution of impactor populations in space and time; (7) an extreme environment in which highly radar-reflective polar deposits, much more extensive than those on the Moon, can be better understood; (8) an extreme environment in which the basic processes of space weathering can be further deduced; and (9) a potential end-member in terrestrial planetary body geological evolution in which the relationships of internal and surface evolution can be clearly assessed from both a tectonic and volcanic point of view. In the half-century since the launch of Sputnik, more than 30 spacecraft have been sent to the Moon, yet only now is a second spacecraft en route to Mercury. The MESSENGER mission will address key questions ...

show abstract

“…Albedo features around 200 km in size have been detected on the non-Mariner 10 hemisphere with the Mt. Wilson 1.5-m reflector (Baumgardner et al 2000) and the Swedish Vacuum Solar Telescope (Warell & Limaye 2001), showing that there is no statistical difference between the morphology and distribution features on a global scale. This provides evidence for a similar post-heavy bombardment geologic evolution of both hemispheres.…”

Section: Important Observational Studiesmentioning

confidence: 97%

Recent Advances in Ground-Based Observation of Mercury

Warell

2005

Highlights astron.

Self Cite

View full text Add to dashboard Cite

R e c e n t A d v a n c e s in G r o u n d -B a s e d O b s e r v a t i o n ofThe last decade has seen an efficient use of ground-based telescopes for remote-sensing studies of Mercury's surface at optical, infrared and microwave wavelengths. This has resulted in a substantially improved knowledge of its regolith composition, material and light scattering properties and structures on the poorly known hemisphere. This paper summarizes recent observations and results on the regolith properties of Mercury.

show abstract

Properties of the Hermean regolith: I. Global regolith albedo variation at 200 scale from multicolor CCD imaging

Cited by 45 publications

References 41 publications

The surface‐bounded atmospheres of Mercury and the Moon

The surface‐bounded atmospheres of Mercury and the Moon

The Geology of Mercury: The View Prior to the MESSENGER Mission

Recent Advances in Ground-Based Observation of Mercury

Contact Info

Product

Resources

About